``Shallow Water'' MHD Waves in the Solar Tachocline

Details ``Shallow Water'' MHD Waves in the Solar Tachocline ``Shallow Water'' MHD Waves in the Solar Tachocline

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sp31a18s&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SP31A-18

Astronomy and Astrophysics

Astrophysics

7500 Solar Physics, Astrophysics, And Astronomy, 7524 Magnetic Fields, 7544 Stellar Interiors And Dynamo Theory

Scientific paper

Peter Gilman recently introduced ``Shallow water'' magnetohydrodynamics (SMHD) as a simple model for understanding predominantly horizontal flows in the solar tachocline. Here, we present analytic solutions to SMHD waves in the tachocline. We show that there are two branches of such waves: Alfvén and magneto-gravity. Finite Alfvén and magneto-gravity waves can both propagate without change of shape in regions of the tachocline where the Coriolis force is finite. At the equator, where the Coriolis force is zero, magneto-gravity waves steepen and develop singularities. We show that the time required for a singularity to develop increases monotonically with the ambient magnetic field strength. Currently, a numerical model is being developed for an extensive study of nonlinear SMHD in the tachocline. This model is based on the β -plane approximation of geophysical fluid dynamics. The β -plane approximation removes some of the complications of spherical geometry, but keeps latitudinal variation in the Coriolis parameter. Early results from this model should be available for this presentation.

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